LIGO s Thermal Noise Interferometer: Progress and Status
|
|
- Brianne Malone
- 5 years ago
- Views:
Transcription
1 LIGO s Thermal Noise Interferometer: Progress and Status Eric Black LSC Meeting Review November 12, 2003 Ivan Grudinin, Akira Villar, Kenneth G. Libbrecht Thanks also to: Kyle Barbary, Adam Bushmaker, Jay Heefner, Fumiko Kawazoe, Luca Matone, Sharon Meidt, Shanti Rao, Kevin Schulz, Michael Zhang Seiji Kawamura
2 Short Term TNI Purpose and Goals Characterize Sapphire for use in Advanced LIGO: Noise Performance, lead time, etc. Contribute to AdvLIGO COC downselect decision. Evaluate thermal noise of coatings for AdvLIGO. Long Term Isolate and study non-gaussian noise in suspensions and mirrors. Reach (and Exceed) the Standard Quantum Limit. Along the way Identify and quantify any unexpected noise sources at sensitivity levels relevant to gravitational-wave detection.
3 TNI Layout
4 TNI Hardware Mode cleaner, arm cavities all contained in one chamber, mounted on a single stack. Wire suspensions similar to LIGO-I Small Optics Suspensions. OSEM actuation, all analog. Laser: 750mW NPRO (Lightwave). All hardware constructed (purchased) and installed.
5 TNI Phase I Expected Spectrum Total Fused-Silica Test Masses Wire Suspensions OSEM Actuation Brownian x ν, m/hz 1/ Radiation Pendulum Thermoelastic Seismic Shot Noise Frequency
6 TNI Phase II Expected Spectrum Total Sapphire Test Masses Wire Suspensions OSEM Actuation x ν, m/hz 1/ Radiation Pendulum Thermoelastic Brownian Seismic Shot Noise Frequency
7 Summer 2001: First data. Schedule: Major Milestones December 2001: SAC noise level approaches scientifically interesting region, ~1e-18 m/ Hz from 1-6 khz, but instrument only locks late at night. NAC noise still high. 2002: Instrument Improvements Improved lock acquisition, stability (robustness). Developing daytime locking capability resulted in loss of sensitivity. Identified, quantified individual noise source contributions. Equalized arm-cavity noise levels. Quality control in photodetectors, beamsplitter; polarization optimization. 2003: Sensitivity Gains, Preliminary Science Results Recovered initial good SAC sensitivity, comparable NAC sensitivity, and retained ability to lock in a challenging seismic environment (MINOS detector assembly next door). Measurement of coating thermal noise on fused silica substrates. March 2004: Provide sapphire data for AdvLIGO COC downselect decision.
8 Latest Sensitivity Curve: 10/23/03 Major improvements since August LSC meeting: Increased modulation depth to suppress photodetector electronic noise. Careful calculation of thermal noise to account for multiple mirrors, difference measurement. Best sensitivity is now approximately 5e-19 m/ Hz. Noise floor appears to be dominated by coating thermal noise from approx. 500 Hz to 20 khz.
9 Calibration δv = DC 1+ DHMC δl To convert the measured voltage into an equivalent length noise, we must know the transfer functions of each servo block. D = Pound-Drever Frequency Discriminant H = Electronic transfer function M = Mirror response (displacement) to signal applied to OSEM controller s FAST-INPUT (voltage) C = Cavity length to frequency conversion factor Specify H and C, verify H by direct measurement. How to determine D and M?
10 Conversion Factor (C) C = ν L = MHz µm This is just math. Converts length change to frequency change. No poles or zeroes, just a number we can calculate. ν = c λ = Hz L =1cm
11 Mirror Response (M): Michelson Measurement Auxilliary Michelson interferometer. Sweep through multiple fringes and count. Rough estimate only!
12 Mirror Response (M): Frequency-Response Measurement Introduce known frequency fluctuation via Laser s PZT. Measure feedback voltage. Well below UGF, transfer function is δf = DH 1+ DHMC δν δν MC Accuracy limited by how well we know the frequency fluctuation δν, which in turn depends on how well we know the laser s PZT response. PZT response measured using reference cavity and known sidebands, ultimately depends on frequency source used to produce sidebands (DS345). Measured PZT response is consistent with manufacturer s spec.
13 Mirror Response (M) Michelson method: Initial rough estimate M 0 () 1 µm V Frequency-response method: Accuracy traceable to commercial frequency reference M 0 ()= µm V Two methods agree. Use frequency-response value for final analysis. NAC and SAC M s are matched to within 7%.
14 Discriminant (D): Sweep Method Direct measurement of Pound-Drever- Hall error signal. Let mirror sweep through a fringe. Identify TEM-00 mode by visibility (not shown in this shot). This is only an estimate of D. D = 2 V t c sb t c 14.75MHz
15 Discriminant (D): UGF Method Measure open-loop transfer function with system locked Fit theory to data New calibration for every lock Blue is data, red is model. One parameter varied for fit: D This method appears to get frequency scaling right. Values obtained are consistent with those obtained by sweep method. Typical: D = 9.0 V MHz Expect: T = DHMC
16 What Causes the Noise Floor? Having established that the instrument is well calibrated, we now want to know the origin of the noise floor. Where in the system does this noise originate? Clues: 1. Incoherence: Differential measurement selects for uncorrelated noise. 2. Scaling with power, modulation depth: True length fluctuations in the arm cavities should be independent of both. Measured voltage should scale linearly with power, product of Bessel functions with modulation depth. Expect δv = RP 0 J 0 ()J β () 1 β 16 F λ δl
17 Power Scaling: δvvs. P 0 Measured voltage noise is proportional to laser power for both high and low modulation depths. Expect this to be true if output voltage is dominated by either Cavity length noise, or Laser frequency noise This measurement rules out the photdetectors or any subsequent measurement electronics as the dominant noise source.
18 Modulation Depth: δvvs. β Discriminant D scales as expected (qualitatively) with modulation depth. Equivalenth length noise in each cavity is independent of modulation depth. Differential noise rises slightly at very low modulation depths due to photodetector electronic noise. Differential noise is only independent of modulation for high-β, where it is quite stable. The noise really is in the cavities, but did it originate there?
19 Servo Noise? Power and modulation-depth scaling indicates that the dominant noise source in the TNI does not come after the cavities in the measurement path. Differential measurement rules out laser frequency noise. Noise must be inside the cavities, but how do we know it originates there? Measure electronic noise going into M, convert to equivalent length noise.
20 Dominant Noise Source is Not Servo Noise
21 What We Have Not Ruled Out 1. OSEM noise: Noise in the local dampers. Mirror transfer function scales as f -2 ; noise floor has f -1/2 dependence. For OSEM noise to be responsible for our noise floor, it would have to have an f +3/2 frequency dependence, which seems unlikely. 2. Thermal noise Pendulum Substrate Coating
22 Pendulum Thermal Noise Pendulum thermal noise theory (above resonant frequency ) S pend ()= f 16k BT 2πf 2 ( ) 5 ω 0 Q pend ω 0 One unknown parameter: Q pend Estimate from similar systems A. Gillespie and F. Raab, Phys. Lett. A, 190, (1994). Music wire with steel clamps, our geometry and loading factor: Q pend
23 Substrate Thermal Noise and Observed Q s Mirror Q s may be determined by localized losses, e.g. Barrel polish (visibly poor) Magnets glued on backs and sides Contact with suspension wires Expect bulk thermal noise to be lower than estimates based on Q measurements Yamamoto, et al., Phys. Lett. A 305, pp (2002) Measured mirror Q s in the TNI range from 1e3 to 3e6. φ substrate = 1 Q < φ substrate < S x () f 2k T B π 32 f 1 ωy φ substrate
24 Q Measurements in Fused Silica Test Masses Q measurements were found to vary from 1700 to over 3 million. Q vs. Frequency for the Fused Silica Mirrors in the TNI 1 E+07 Q (unitless) 1 E+06 1 E+05 1 E+04 NAC Input NAC Output SAC Input SAC Output 1 E Frequency (khz)
25 Coating Thermal Noise Coating thermal noise, best estimate Crooks, et al., Class. Quantum Grav. 19 (5) pp (2002) Harry et al., Class. Quantum Grav. 19 (5) pp (2002) S x ()= f 8k BT π 32 f ~ k BT ωyf 1 ωy φ coating >> ω d φ substrate φ + 1 d Y substrate π ω Y φ + Y Y φ φ substrate + d ω φ coating φ Ringdown coating-q measurements give, but only direct measurement can give? Condition required to distinguish coating thermal noise from substrate thermal noise: For the TNI, ω d 160µm 5µm = 32 φ Expect: φ coating ~ φ substrate Condition met by factor of ten in TNI.
26 TNI Noise Breakdown
27 Next Step: Sapphire Substrates
28 Conclusions TNI noise floor appears to be dominated by coating thermal noise from 500 Hz to 20 khz. Losses in these SiO 2 /Ta 2 O 5 coatings appear to be isotropic: Ringdown measurements give We obtain by experimental fit to our data φ φ φ = φ = TNI is on track for April 2004 AdLIGO COC material downselect. Deadline for thermal noise measurement with fused-silica mirrors was Oct. 29. Our measurement was completed Oct. 23. Current noise floor is below predicted Sapphire noise from 400 Hz to 4 khz. Expect coating thermal noise to go down due to increased Young s modulus of substrate. Will it?
An Overview of Advanced LIGO Interferometry
An Overview of Advanced LIGO Interferometry Luca Matone Columbia Experimental Gravity group (GECo) Jul 16-20, 2012 LIGO-G1200743 Day Topic References 1 2 3 4 5 Gravitational Waves, Michelson IFO, Fabry-Perot
More information6WDWXVRI/,*2. Laser Interferometer Gravitational-wave Observatory. Nergis Mavalvala MIT IAU214, August 2002 LIGO-G D
6WDWXVRI/,*2 Laser Interferometer Gravitational-wave Observatory Hanford, WA Livingston, LA Nergis Mavalvala MIT IAU214, August 2002 *UDYLWDWLRQDOZDYH,QWHUIHURPHWHUVWKHSULQ LSOH General Relativity (Einstein
More informationThe Status of Enhanced LIGO.
The Status of Enhanced LIGO. Aidan Brooks. December 2008 AIP Congress 2008, Adelaide, Australia 1 Outline Gravitational Waves» Potential sources» Initial LIGO interferometer Enhanced LIGO upgrades» Increased
More informationStatus and Plans for Future Generations of Ground-based Interferometric Gravitational-Wave Antennas
Status and Plans for Future Generations of Ground-based Interferometric Gravitational-Wave Antennas 4 th international LISA Symposium July 22, 2002 @ Penn State University Seiji Kawamura National Astronomical
More informationThe Advanced LIGO detectors at the beginning of the new gravitational wave era
The Advanced LIGO detectors at the beginning of the new gravitational wave era Lisa Barsotti MIT Kavli Institute LIGO Laboratory on behalf of the LIGO Scientific Collaboration LIGO Document G1600324 LIGO
More informationDevelopment of ground based laser interferometers for the detection of gravitational waves
Development of ground based laser interferometers for the detection of gravitational waves Rahul Kumar ICRR, The University of Tokyo, 7 th March 2014 1 Outline 1. Gravitational waves, nature & their sources
More informationExperimental measurements of coating mechanical loss factors
INSTITUTE OF PHYSICS PUBLISHING Class. Quantum Grav. 21 (2004) S1059 S1065 CLASSICAL AND QUANTUM GRAVITY PII: S0264-9381(04)69009-5 Experimental measurements of coating mechanical loss factors D R M Crooks
More informationAdvanced LIGO Research and Development
Advanced LIGO Research and Development David Shoemaker NSF Annual Review of LIGO 17 November 2003 LIGO Laboratory 1 LIGO mission: detect gravitational waves and initiate GW astronomy Commissioning talk
More informationAfter ~ 40 years of effort, no one has detected a GW! Why? Noise levels in detectors exceed expected
NOISE in GW detectors After ~ 40 years of effort, no one has detected a GW! Why? Noise levels in detectors exceed expected signal; insufficient sensitivity Want to detect GW strain h; can express detector
More informationThermal noise from optical coatings in gravitational wave detectors
Thermal noise from optical coatings in gravitational wave detectors Gregory M. Harry, Helena Armandula, Eric Black, D. R. M. Crooks, Gianpietro Cagnoli, Jim Hough, Peter Murray, Stuart Reid, Sheila Rowan,
More informationAdvanced LIGO, Advanced VIRGO and KAGRA: Precision Measurement for Astronomy. Stefan Ballmer For the LVC Miami 2012 Dec 18, 2012 LIGO-G
Advanced LIGO, Advanced VIRGO and KAGRA: Precision Measurement for Astronomy Stefan Ballmer For the LVC Miami 2012 Dec 18, 2012 LIGO-G1201293 Outline Introduction: What are Gravitational Waves? The brief
More informationDisplacement Noises in Laser Interferometric Gravitational Wave Detectors
Gravitational Wave Physics @ University of Tokyo Dec 12, 2017 Displacement Noises in Laser Interferometric Gravitational Wave Detectors Yuta Michimura Department of Physics, University of Tokyo Slides
More informationStatus of LIGO. David Shoemaker LISA Symposium 13 July 2004 LIGO-G M
Status of LIGO David Shoemaker LISA Symposium 13 July 2004 Ground-based interferometric gravitational-wave detectors Search for GWs above lower frequency limit imposed by gravity gradients» Might go as
More informationAdvanced LIGO Status Report
Advanced LIGO Status Report Gregory Harry LIGO/MIT On behalf of the LIGO Science Collaboration 22 September 2005 ESF PESC Exploratory Workshop Perugia Italy LIGO-G050477 G050477-00-R Advanced LIGO Overview
More informationPresent and Future. Nergis Mavalvala October 09, 2002
Gravitational-wave Detection with Interferometers Present and Future Nergis Mavalvala October 09, 2002 1 Interferometric Detectors Worldwide LIGO TAMA LISA LIGO VIRGO GEO 2 Global network of detectors
More informationNext Generation Interferometers
Next Generation Interferometers TeV 06 Madison Rana Adhikari Caltech 1 Advanced LIGO LIGO mission: detect gravitational waves and initiate GW astronomy Next detector» Should have assured detectability
More informationSearching for Stochastic Gravitational Wave Background with LIGO
Searching for Stochastic Gravitational Wave Background with LIGO Vuk Mandic University of Minnesota 09/21/07 Outline LIGO Experiment:» Overview» Status» Future upgrades Stochastic background of gravitational
More informationHow to measure a distance of one thousandth of the proton diameter? The detection of gravitational waves
How to measure a distance of one thousandth of the proton diameter? The detection of gravitational waves M. Tacca Laboratoire AstroParticule et Cosmologie (APC) - Paris Journée GPhys - 2016 July 6th General
More informationMaximum heat transfer along a sapphire suspension fiber for a cryogenic interferometric gravitational wave detector
Maximum heat transfer along a sapphire suspension fiber for a cryogenic interferometric gravitational wave detector T. Tomaru 1, T. Suzuki, T. Uchiyama, A. Yamamoto, T. Shintomi High Energy Accelerator
More informationSqueezed Light for Gravitational Wave Interferometers
Squeezed Light for Gravitational Wave Interferometers R. Schnabel, S. Chelkowski, H. Vahlbruch, B. Hage, A. Franzen, and K. Danzmann. Institut für Atom- und Molekülphysik, Universität Hannover Max-Planck-Institut
More informationMeasurements of the optical mirror coating properties.
Measurements of the optical mirror coating properties. V.B. Braginsky, A.A. Samoilenko Dept. of Phys. Moscow State University Moscow 119992, Russia. arxiv:gr-qc/0304100v1 29 Apr 2003 February 5, 2008 Abstract
More informationGravitational Wave Detection from the Ground Up
Gravitational Wave Detection from the Ground Up Peter Shawhan (University of Maryland) for the LIGO Scientific Collaboration LIGO-G080393-00-Z From Simple Beginnings Joe Weber circa 1969 AIP Emilio Segre
More informationA MODERN MICHELSON-MORLEY EXPERIMENT USING ACTIVELY ROTATED OPTICAL RESONATORS
A MODERN MICHELSON-MORLEY EXPERIMENT USING ACTIVELY ROTATED OPTICAL RESONATORS S. HERRMANN, A. SENGER, K. MÖHLE, E. V. KOVALCHUK, A. PETERS Institut für Physik, Humboldt-Universität zu Berlin Hausvogteiplatz
More informationAdvanced LIGO Research and Development
Advanced LIGO Research and Development David Shoemaker NSF Annual Review of LIGO 17 October 2003 LIGO Laboratory 1 LIGO mission: detect gravitational waves and initiate GW astronomy Commissioning talk
More informationProgress in Gravitational Wave Detection: Interferometers
1 Progress in Gravitational Wave Detection: Interferometers Kazuaki Kuroda a and LCGT Collaboration b a Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba 277-8582,
More informationGEO 600: Advanced Techniques in Operation
GEO 600: Advanced Techniques in Operation Katherine Dooley for the GEO team DCC# G1400554-v1 LISA Symposium X Gainesville, FL May 21, 2014 GEO600 Electronics shop Corner building Operator's station Offices
More informationInterferometric. Gravitational Wav. Detectors. \p World Scientific. Fundamentals of. Peter R. Sawlson. Syracuse University, USA.
SINGAPORE HONGKONG Fundamentals of Interferometric Gravitational Wav Detectors Second Edition Peter R. Sawlson Martin A. Pomerantz '37 Professor of Physics Syracuse University, USA \p World Scientific
More informationSilica research in Glasgow
INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 1655 1662 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)29440-X Silica research in Glasgow BWBarr 1, G Cagnoli 1,7,MMCasey 1, D Clubley 1,
More informationPhasor Calculations in LIGO
Phasor Calculations in LIGO Physics 208, Electro-optics Peter Beyersdorf Document info Case study 1, 1 LIGO interferometer Power Recycled Fabry-Perot Michelson interferometer 10m modecleaner filters noise
More informationFused silica suspension for the Virgo optics: status and perspectives
Fused silica suspension for the Virgo optics: status and perspectives Helios Vocca for the Virgo Perugia Group The expected Virgo Sensitivity 10-15 Total sensitivity h(f) [1/sqrt(Hz)] 10-16 10-17 10-18
More informationAdvanced Virgo: Status and Perspectives. A.Chiummo on behalf of the VIRGO collaboration
Advanced Virgo: Status and Perspectives A.Chiummo on behalf of the VIRGO collaboration Advanced Virgo 2 Advanced Virgo What s that? 3 Advanced Virgo Advanced Virgo (AdV): upgrade of the Virgo interferometric
More informationLIGO I status and advanced LIGO proposal
LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech LIGO I» basic design» current status advanced LIGO» outline of the proposal» technical issues GW signals and data analysis ICRR
More informationAdvanced LIGO Optical Configuration and Prototyping Effort
Advanced LIGO Optical Configuration and Prototyping Effort Alan Weinstein *, representing the LIGO Scientific Collaboration Advanced Interferometer Configurations Working Group, and the LIGO 40 Meter Group
More informationBASELINE SUSPENSION DESIGN FOR LIGO II - UPDATE
BASELINE SUSPENSION DESIGN FOR LIGO II - UPDATE Norna A Robertson University of Glasgow for the GEO suspension team LSC, Hanford 15th August 2000 LIGO-G000295-00-D GEO suspension team for LIGO II G Cagnoli,
More informationGravitational Wave Astronomy
Gravitational Wave Astronomy Giles Hammond SUPA, University of Glasgow, UK on behalf of the LIGO Scientific Collaboration and the Virgo Collaboration 14 th Lomonosov conference on Elementary Particle Physics
More informationLIGO: The Laser Interferometer Gravitational Wave Observatory
LIGO: The Laser Interferometer Gravitational Wave Observatory Credit: Werner Benger/ZIB/AEI/CCT-LSU Michael Landry LIGO Hanford Observatory/Caltech for the LIGO Scientific Collaboration (LSC) http://www.ligo.org
More informationLASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Document Type LIGO-T960148-01- D Sep / 9 / 96 Maximum Current of the
More informationThe gravitational wave detector VIRGO
The gravitational wave detector VIRGO for the VIRGO collaboration Raffaele Flaminio Laboratoire d Annecy-le-Vieux de Physique des Particules (LAPP) IN2P3 - CNRS Summary I. A bit of gravitational wave physics
More informationLIGO ADVANCED SYSTEMS TEST INTERFEROMETER (LASTI)
LIGO ADVANCED SYSTEMS TEST INTERFEROMETER (LASTI) Program Update: LSC Meeting, Hannover Dave Ottaway August 2003 LSC Meeting August 03 1 Talk Overview 1. LASTI goals and timelines 2. Overview of progress
More informationGROUND NOISE STUDIES USING THE TAMA300 GRAVITATIONAL-WAVE DETECTOR AND RELATED HIGHLY-SENSITIVE INSTRUMENTS
GROUND NOISE STUDIES USING THE TAMA300 GRAVITATIONAL-WAVE DETECTOR AND RELATED HIGHLY-SENSITIVE INSTRUMENTS Akito ARAYA Earthquake Research Institute, University of Tokyo, 1-1-1, Yayoi, Bunkyo, Tokyo 113-0032,
More informationExcess mechanical loss associated with dielectric mirror coatings on test masses in
Home Search Collections Journals About Contact us My IOPscience Excess mechanical loss associated with dielectric mirror coatings on test masses in interferometric gravitational wave detectors This article
More informationStudy of a quantum nondemolition interferometer using ponderomotive squeezing
Study of a quantum nondemolition interferometer using ponderomotive squeezing Ochanomizu University, National Astronomical Observatory of Japan A, and Max-Planck-Institut für Gravitationsphysik B Shihori
More informationGravitational Waves and LIGO
Gravitational Waves and LIGO Ray Frey, University of Oregon 1. GW Physics and Astrophysics 2. How to detect GWs The experimental challenge 3. Prospects June 16, 2004 R. Frey QNet 1 General Relativity Some
More informationAdvanced Virgo and LIGO: today and tomorrow
Advanced Virgo and LIGO: today and tomorrow Michał Was for the LIGO and Virgo collaborations Michał Was (SFP Gravitation) 2017 Nov 22 1 / 21 d Basics of interferometric gravitational wave detections Need
More informationGravitational Waves and LIGO: A Technical History
Gravitational Waves and LIGO: A Technical History Stan Whitcomb IEEE SV Tech History Committee Event 11 October 2018 LIGO-G180195-v3 Goal of Talk Review a few of the technical developments that enabled
More informationRecent LIGO I simulation results
Recent LIGO I simulation results Hiro Yamamoto / Caltech - LIGO Lab As-built LIGO I performance and the path to it FFT run with as-built HR phase map» Contrast defect» Shot noise limited sensitivity» R.Dodda(SLU),
More informationKeywords: Fabry Perot cavity; radiation pressure; feedback; gravitational waves.
General Relativity and Gravitation Manuscript Draft Manuscript Number: GERG-D-07-00020 Title: Radiation pressure effects in the Virgo input mode cleaner Article Type: Original Research Keywords: Fabry
More informationThe Quantum Limit and Beyond in Gravitational Wave Detectors
The Quantum Limit and Beyond in Gravitational Wave Detectors Gravitational wave detectors Quantum nature of light Quantum states of mirrors Nergis Mavalvala GW2010, UMinn, October 2010 Outline Quantum
More informationThe status of VIRGO. To cite this version: HAL Id: in2p
The status of VIRGO E. Tournefier, F. Acernese, P. Amico, M. Al-Shourbagy, S. Aoudia, S. Avino, D. Babusci, G. Ballardin, R. Barillé, F. Barone, et al. To cite this version: E. Tournefier, F. Acernese,
More informationLIGO Status Report 1. LIGO I. 2. E7 run (Dec.28,2001 ~ Jan.14,2002) 3. Advanced LIGO. Hiro Yamamoto
LIGO Status Report Hiro Yamamoto LIGO Laboratory / California Institute of Technology 1. LIGO I 2. E7 run (Dec.28,2001 ~ Jan.14,2002) 3. Advanced LIGO References : M.Coles (G020009), D.Coyne and D.Shoemaker
More informationPhysics of LIGO Lecture 2
Last week: LIGO project GW physics, astrophysical sources Principles of GW IFO s This week: Engineering and Science runs Noise in GW IFOs Focus on thermal noise Next week: Optics Control systems Advanced
More informationProbing for Gravitational Waves
Probing for Gravitational Waves LIGO Reach with LIGO AdLIGO Initial LIGO Barry C. Barish Caltech YKIS2005 Kyoto University 1-July-05 Einstein s Theory of Gravitation a necessary consequence of Special
More informationInterferometry beyond the Standard Quantum Limit using a Sagnac Speedmeter Stefan Hild
Interferometry beyond the Standard Quantum Limit using a Sagnac Speedmeter Stefan Hild ET general meeting Hannover, December 2012 Overview Ü What is a speedmeter and how does it work? Ü Could a Sagnac
More informationLIGO: On the Threshold of Gravitational-wave Astronomy
LIGO: On the Threshold of Gravitational-wave Astronomy Stan Whitcomb LIGO/Caltech IIT, Kanpur 18 December 2011 Outline of Talk Quick Review of GW Physics and Astrophysics LIGO Overview» Initial Detectors»
More informationOverview Ground-based Interferometers. Barry Barish Caltech Amaldi-6 20-June-05
Overview Ground-based Interferometers Barry Barish Caltech Amaldi-6 20-June-05 TAMA Japan 300m Interferometer Detectors LIGO Louisiana 4000m Virgo Italy 3000m AIGO Australia future GEO Germany 600m LIGO
More informationThe Quest to Detect Gravitational Waves
The Quest to Detect Gravitational Waves Peter Shawhan California Institute of Technology / LIGO Laboratory What Physicists Do lecture Sonoma State University March 8, 2004 LIGO-G040055-00-E Outline Different
More informationExcess Mechanical Loss Associated with Dielectric Mirror Coatings on Test Masses in Interferometric Gravitational Wave Detectors
Excess Mechanical Loss Associated with Dielectric Mirror Coatings on Test Masses in Interferometric Gravitational Wave Detectors D. R. M. Crooks, P. Sneddon, G. Cagnoli, J. Hough Dept of Physics and Astronomy
More informationStatus and Prospects for LIGO
Status and Prospects for LIGO Crab Pulsar St Thomas, Virgin Islands Barry C. Barish Caltech 17-March-06 LIGO Livingston, Louisiana 4 km 17-March-06 Confronting Gravity - St Thomas 2 LIGO Hanford Washington
More informationTowards Sagnac speed meter interferometers for gravitational wave detection
Towards Sagnac speed meter interferometers for gravitational wave detection Christian Gräf for the Glasgow Sagnac Speed Meter Team ICONO/LAT Conference, September 2016 Minsk, Belarus LIGO-G1601997 Outline
More informationLIGO On-line Documents July 1997
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Document Type LIGO-T970089-05- P 7/22/97 LIGO On-line Documents July
More informationAdvanced LIGO Optical Configuration, Prototyping, and Modeling
Advanced LIGO Optical Configuration, Prototyping, and Modeling Alan Weinstein *, representing the LIGO Scientific Collaboration Advanced Interferometer Configurations Working Group, and the LIGO 40 Meter
More informationarxiv:gr-qc/ v1 12 Feb 2002
Thermal lensing in cryogenic sapphire substrates arxiv:gr-qc/0202038v1 12 Feb 2002 Takayuki Tomaru, Toshikazu Suzuki, Shinji Miyoki, Takashi Uchiyama, C.T. Taylor, Akira Yamamoto, Takakazu Shintomi, Masatake
More informationGearing up for Gravitational Waves: the Status of Building LIGO
Gearing up for Gravitational Waves: the Status of Building LIGO Frederick J. Raab, LIGO Hanford Observatory LIGO s Mission is to Open a New Portal on the Universe In 1609 Galileo viewed the sky through
More informationThermal Corrective Devices for Advanced Gravitational Wave Interferometers
Thermal Corrective Devices for Advanced Gravitational Wave Interferometers Marie Kasprzack, Louisiana State University 6 th October 2016 COMSOL Conference 2016 Boston 1 1. Advanced Gravitational Wave Detectors
More informationPhysics of LIGO Lecture 3
Physics of LIGO Lecture 3 Last week: LIGO project GW physics, astrophysical sources Principles of GW IFO s Engineering and Science runs Noise in GW IFOs Focus on thermal noise This week: Cavity Optics
More informationResonances, quality factors in LIGO pendulums: a compendium of formulas
Resonances, quality factors in LIGO pendulums: a compendium of formulas Gabriela González December 11, 2001 1 Introduction and notes There are simple formulas for the different pendulum and violin modes,
More informationOptical Coatings and Thermal Noise in Precision Measurements
Optical Coatings and Thermal Noise in Precision Measurements Embry-Riddle Aeronautical University Physics Colloquium October 25, 2011 Gregory Harry American University LIGO-G1101150 Thermal Noise Random
More informationObservation of reduction of radiation-pressure-induced rotational anti-spring effect on a 23 mg
Home Search Collections Journals About Contact us My IOPscience Observation of reduction of radiation-pressure-induced rotational anti-spring effect on a 23 mg mirror in a Fabry Perot cavity This content
More informationPlans for Advanced Virgo
Plans for Advanced Virgo Raffaele Flaminio Laboratoire des Materiaux Avances CNRS/IN2P3 On behalf of the Virgo-IN2P3 groups (APC, LAL, LAPP, LMA) SUMMARY - Scientific case - Detector design - The IN2P3
More information! How to design feedback filters! for a given system?!!
How to design feedback filters for a given system? October 3, 3 Osamu Miyakawa Seminar at Kamioka Brach, October 3 Requirement : Assumption of Linearity Carrier Requirement : Control theory assumes linearity.
More informationLIGO workshop What Comes Next for LIGO May 7-8, 2015, Silver Spring, MD KAGRA KAGRA. Takaaki Kajita, ICRR, Univ. of Tokyo for the KAGRA collaboration
LIGO workshop What Comes Next for LIGO May 7-8, 2015, Silver Spring, MD KAGRA KAGRA Takaaki Kajita, ICRR, Univ. of Tokyo for the KAGRA collaboration Outline Introduction: Overview of KAGRA Status of the
More informationAdvanced LIGO: Context and Overview
Advanced LIGO Advanced LIGO: Context and Overview Gravitational waves offer a remarkable opportunity to see the universe from a new perspective, providing access to astrophysical insights that are available
More informationFile name: Supplementary Information Description: Supplementary Figures, Supplementary Notes and Supplementary References
File name: Supplementary Information Description: Supplementary Figures, Supplementary Notes and Supplementary References File name: Peer Review File Description: Optical frequency (THz) 05. 0 05. 5 05.7
More informationarxiv:gr-qc/ v1 4 Dec 2003
Testing the LIGO Inspiral Analysis with Hardware Injections arxiv:gr-qc/0312031 v1 4 Dec 2003 Duncan A. Brown 1 for the LIGO Scientific Collaboration 1 Department of Physics, University of Wisconsin Milwaukee,
More informationLaser Interferometer Gravitationalwave Observatory LIGO Industrial Physics Forum. Barry Barish 7 November 2000 LIGO-G9900XX-00-M
Laser Interferometer Gravitationalwave Observatory LIGO 2000 Industrial Physics Forum Barry Barish 7 November 2000 Sir Isaac Newton Perhaps the most important scientist of all time! Invented the scientific
More informationMechanical Q-factor measurements on a test mass with a structured surface
Mechanical Q-factor measurements on a test mass with a structured surface To cite this article: R Nawrodt et al 2007 New J. Phys. 9 225 View the article online for updates and enhancements. Related content
More informationarxiv: v2 [gr-qc] 14 Mar 2012
Detector configuration of KAGRA - the Japanese cryogenic gravitational-wave detector - arxiv:1111.7185v [gr-qc] 14 Mar 01 Kentaro Somiya (for the KAGRA Collaboration) Graduate School of Science and Technology,
More informationSqueezed states of light - generation and applications
Squeezed states of light - generation and applications Eugeniy E. Mikhailov The College of William & Mary Fudan, December 24, 2013 Eugeniy E. Mikhailov (W&M) Squeezed light Fudan, December 24, 2013 1 /
More informationAdvanced Virgo: status and gravitational waves detection. Flavio Travasso on behalf of Virgo Collaboration INFN Perugia - University of Perugia - EGO
Advanced Virgo: status and gravitational waves detection Flavio Travasso on behalf of Virgo Collaboration INFN Perugia - University of Perugia - EGO Minkowski vs general metric dx dx ds 2 1 1 1 1 Flat
More informationReview of LIGO Upgrade Plans
Ando Lab Seminar April 13, 2017 Review of LIGO Upgrade Plans Yuta Michimura Department of Physics, University of Tokyo Contents Introduction A+ Voyager Cosmic Explorer Other issues on ISC Summary KAGRA+
More informationThe gravitational waves detection: 20 years of research to deliver the LIGO/VIRGO mirrors. Christophe MICHEL on behalf of LMA Team
Christophe MICHEL on behalf of LMA Team 1 The event February 11th 2016 LIGO and VIRGO announced the first direct detection of gravitational waves https://www.youtube.com/watch?v=vd1pak5f6gq http://journals.aps.org/prl/abstract/10.1103/physrevlett.1
More informationThe technology behind LIGO: how to measure displacements of meters
The technology behind LIGO: how to measure displacements of 10-19 meters The LIGO interferometers Interferometry: displacement sensing Noise limits Advanced LIGO 4pm today, 1 West: Results from science
More informationSqueezed Light Techniques for Gravitational Wave Detection
Squeezed Light Techniques for Gravitational Wave Detection July 6, 2012 Daniel Sigg LIGO Hanford Observatory Seminar at TIFR, Mumbai, India G1200688-v1 Squeezed Light Interferometry 1 Abstract Several
More informationSqueezing manipulation with atoms
Squeezing manipulation with atoms Eugeniy E. Mikhailov The College of William & Mary March 21, 2012 Eugeniy E. Mikhailov (W&M) Squeezing manipulation LSC-Virgo (March 21, 2012) 1 / 17 About the college
More informationAdvanced LIGO, LIGO-Australia and the International Network
Advanced LIGO, LIGO-Australia and the International Network Stan Whitcomb LIGO/Caltech IndIGO - ACIGA meeting on LIGO-Australia 8 February 2011 Gravitational Waves Einstein in 1916 and 1918 recognized
More informationActive Isolation and Alignment in 6 DOF for LIGO 2
Active Isolation and Alignment in 6 DOF for LIGO 2 JILA, LSU, MIT, Stanford LIGO Science Collaboration Rana Adhikari, Graham Allen, Daniel Debra, Joe Giaime, Giles Hammond, Corwin Hardham, Jonathan How,
More informationLASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY. LIGO Scientific Collaboration. Enhanced LIGO. R Adhikari. Distribution of this draft:
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY LIGO LIGO Scientific Collaboration LIGO T06009-00-I May 006 Enhanced LIGO R Adhikari Distribution of this draft: LIGO Scientific Collaboration This is
More informationVibration-Free Pulse Tube Cryocooler System for Gravitational Wave Detectors I
1 Vibration-Free Pulse Tube Cryocooler System for Gravitational Wave Detectors I - Vibration-Reduction Method and Measurement - T. Tomaru A, T. Suzuki A, T. Haruyama A, T. Shintomi A, N. Sato A, A. Yamamoto
More informationThe Advanced LIGO Gravitational Wave Detector arxiv: v1 [gr-qc] 14 Mar Introduction
The Advanced LIGO Gravitational Wave Detector arxiv:1103.2728v1 [gr-qc] 14 Mar 2011 S. J. Waldman, for the LIGO Scientific Collaboration LIGO Laboratory, Kavli Institute for Astrophysics and Space Research,
More informationEnhancing sensitivity of gravitational wave antennas, such as LIGO, via light-atom interaction
Enhancing sensitivity of gravitational wave antennas, such as LIGO, via light-atom interaction Eugeniy E. Mikhailov The College of William & Mary, USA New Laser Scientists, 4 October 04 Eugeniy E. Mikhailov
More informationLIGO s Detection of Gravitational Waves from Two Black Holes
LIGO s Detection of Gravitational Waves from Two Black Holes Gregory Harry Department of Physics, American University February 17,2016 LIGO-G1600274 GW150914 Early History of Gravity Aristotle Kepler Laplace
More informationTemperature coefficient of refractive index of sapphire substrate at cryogenic temperature for interferometric gravitational wave detectors
Temperature coefficient of refractive index of sapphire substrate at cryogenic temperature for interferometric gravitational wave detectors T. Tomaru, T. Uchiyama, C. T. Taylor, S. Miyoki, M. Ohashi, K.
More informationThe Investigation of Geometric Anti-springs Applied to Euler Spring Vibration Isolators
The Investigation of Geometric Anti-springs Applied to Euler Spring Vibration Isolators Eu-Jeen Chin Honours 2002 School of Physics Supervisors: Prof. David Blair Dr. Li Ju Dr. John Winterflood The University
More informationDIODE LASER SPECTROSCOPY
DIODE LASER SPECTROSCOPY Spectroscopy, and Much More, Using Modern Optics Observe Doppler-Free Spectroscopy of Rubidium Gas Michelson Interferometer Used to Calibrate Laser Sweep Observe Resonant Faraday
More informationTakaaki Kajita, JGRG 22(2012) Status of KAGRA RESCEU SYMPOSIUM ON GENERAL RELATIVITY AND GRAVITATION JGRG 22. November
Takaaki Kajita, JGRG 22(2012)111402 Status of KAGRA RESCEU SYMPOSIUM ON GENERAL RELATIVITY AND GRAVITATION JGRG 22 November 12-16 2012 Koshiba Hall, The University of Tokyo, Hongo, Tokyo, Japan RESCEU
More informationThe LIGO Experiment Present and Future
The LIGO Experiment Present and Future Keith Riles University of Michigan For the LIGO Scientific Collaboration APS Meeting Denver May 1 4, 2004 LIGO-G040239-00-Z What are Gravitational Waves? Gravitational
More informationApril 21-23, Barry Barish LIGO-G M
LIGO NSF Review April 21-23, 1999 Overview Barry Barish LIGO Plans main activity 1996 Construction Underway -mostly civil 1997 Facility Construction -vacuum system 1998 Interferometer Construction -complete
More informationProspects for joint transient searches with LOFAR and the LSC/Virgo gravitational wave interferometers
Prospects for joint transient searches with LOFAR and the LSC/Virgo gravitational wave interferometers Ed Daw - University of Sheffield On behalf of the LIGO Scientific Collaboration and the Virgo collaboration
More informationTHERMAL NOISE IN LOW LOSS FLEXURES
THERMAL NOISE IN LOW LOSS FLEXURES by Andri Marcus Gretarsson BSc. University of Edinburgh, 1995 M.S. Syracuse University, 2000 Dissertation Submitted in partial fulfillment of the requirements for the
More informationLong-term strategy on gravitational wave detection from European groups
Longterm strategy on gravitational wave detection from European groups Barry Barish APPEC Meeting London, UK 29Jan04 International Interferometer Network Simultaneously detect signal (within msec) LIGO
More information